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Very High Energy Observations of Gamma-Ray Burst Locations with the Whipple Telescope D Physics Physics Research Publications Purdue University Year 2007 Very high energy observations of gamma-ray burst locations with the whipple telescope D. Horan, R. W. Atkins, H. M. Badran, G. Blaylock, S. M. Bradbury, J. H. Buckley, K. L. Byrum, O. Celik, Y. C. K. Chow, P. Cogan, W. Cui, M. K. Daniel, I. D. Perez, C. Dowdall, A. D. Falcone, D. J. Fegan, S. J. Fegan, J. P. Finley, P. Fortin, L. F. Fortson, G. H. Gillanders, J. Grube, K. J. Gutierrez, J. Hall, D. Hanna, J. Holder, S. B. Hughes, T. B. Humensky, G. E. Kenny, M. Kertzman, D. B. Kieda, J. Kildea, H. Krawczynski, F. Krennrich, M. J. Lang, S. LeBohec, G. Maier, P. Moriarty, T. Nagal, R. A. Ong, J. S. Perkins, D. Petry, J. Quinn, M. Quinn, K. Ragan, P. T. Reynolds, H. J. Rose, M. Schroedter, G. H. Sembroski, D. Steele, S. P. Swordy, J. A. Toner, L. Valcarcel, V. V. Vassiliev, R. G. Wagner, S. P. Wakely, T. C. Weekes, R. J. White, and D. A. Williams This paper is posted at Purdue e-Pubs. http://docs.lib.purdue.edu/physics articles/357 The Astrophysical Journal, 655:396Y405, 2007 January 20 A # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. VERY HIGH ENERGY OBSERVATIONS OF GAMMA-RAY BURST LOCATIONS WITH THE WHIPPLE TELESCOPE D. Horan,1 R. W. Atkins,2 H. M. Badran,3 G. Blaylock,4 S. M. Bradbury,5 J. H. Buckley,6 K. L. Byrum,7 O. Celik,8 Y. C. K. Chow,8 P. Cogan,9 W. Cui,10 M. K. Daniel,9 I. de la Calle Perez,11 C. Dowdall,9 A. D. Falcone,12 D. J. Fegan,9 S. J. Fegan,8 J. P. Finley,10 P. Fortin,13 L. F. Fortson,14 G. H. Gillanders,15 J. Grube,5 K. J. Gutierrez,6 J. Hall,2 D. Hanna,16 J. Holder,5 S. B. Hughes,6 T. B. Humensky,17 G. E. Kenny,15 M. Kertzman,18 D. B. Kieda,2 J. Kildea,16 H. Krawczynski,6 F. Krennrich,19 M. J. Lang,15 S. LeBohec,2 G. Maier,5 P. Moriarty,20 T. Nagai,19 R. A. Ong,8 J. S. Perkins,6 D. Petry,21 J. Quinn,9 M. Quinn,20 K. Ragan,16 P. T. Reynolds,22 H. J. Rose,5 M. Schroedter,19 G. H. Sembroski,10 D. Steele,14 S. P. Swordy,17 J. A. Toner,15 L. Valcarcel,16 V. V. Vassiliev,8 R. G. Wagner,7 S. P. Wakely,17 T. C. Weekes,1 R. J. White,5 and D. A. Williams23 Received 2006 April 26; accepted 2006 September 15 ABSTRACT Gamma-ray burst (GRB) observations at very high energies (VHE; E > 100 GeV) can impose tight constraints on some GRB emission models. Many GRB afterglow models predict a VHE component similar to that seen in blazars and plerions, in which the GRB spectral energy distribution has a double-peaked shape extending into the VHE re- gime. VHE emission coincident with delayed X-ray flare emission has also been predicted. GRB follow-up obser- vations have had high priority in the observing program at the Whipple 10 m gamma-ray telescope, and GRBs will continue to be high-priority targets as the next-generation observatory, VERITAS, comes online. Upper limits on the VHE emission at late times (>4 hr) from seven GRBs observed with the Whipple Telescope are reported here. Subject headinggs: gamma rays: bursts — gamma rays: observations Online material: color figures 1. INTRODUCTION been found to have fluences ranging from a small fraction of, Since their discovery in 1969 (Klebesadel et al. 1973), gamma- up to a value comparable to, that contained in the prompt GRB emission. This X-ray flare emission has been postulated to arise ray bursts (GRBs) have been well studied at many wavelengths. from a number of different scenarios, including late central en- Although various open questions remain regarding their nature, there is almost universal agreement that the basic mechanism is gine activity, where the GRB progenitor remains active for some time after, or reactivates after, the initial explosion (Kumar & an expanding relativistic fireball, that the radiation is beamed, that Piran 2000; Zhang et al. 2006; Nousek et al. 2006; Perna et al. the prompt emission is due to internal shocks, and that the after- 2006; Proga & Zhang 2006; King et al. 2005), and refreshed glow arises from external shocks. It is likely that Lorentz factors shocks, which occur when slower moving shells ejected by the of a few hundred are involved, with the radiating particles, either central engine in the prompt phase catch up with the afterglow electrons or protons, being accelerated to very high energies. shock at late times (Rees & Me´sza´ros 1998; Sari & Me´sza´ros GRBs are subclassified into two categories, long and short burst, 2000; Granot et al. 2003; Guetta et al. 2007). For short GRBs, based on the timescale over which 90% of the prompt gamma- shock heating of a binary stellar companion has also been pro- rayemissionisdetected. posed (MacFadyen et al. 2005). It is not yet clear whether the Recently, the Swift GRB Explorer (Gehrels et al. 2004) has revealed that many GRBs have associated X-ray flares (Burrows X-ray flares are the result of prolonged central engine activity, refreshed shocks, or some other mechanism (Panateiscu et al. et al. 2005; Falcone et al. 2006). These flares have been detected 2006). A very high energy (VHE; E > 100 GeV) component of between 102 and 105 s after the initial prompt emission and have 1 Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for 13 Department of Physics and Astronomy, Barnard College, Columbia Astrophysics, Amado, AZ; Current address: Argonne National Laboratory, University, NY. Argonne IL. 14 Department of Astronomy, Adler Planetarium and Astronomy Museum, 2 Department of Physics, University of Utah, Salt Lake City, UT. Chicago, IL. 3 Department of Physics, Tanta University, Tanta, Egypt. 15 Department of Physics, National University of Ireland, Galway, Ireland. 4 Department of Physics, University of Massachusetts, Amherst, MA. 16 Department of Physics, McGill University, Montreal, Canada. 5 School of Physics and Astronomy, University of Leeds, Leeds, UK. 17 Enrico Fermi Institute, University of Chicago, Chicago, IL. 6 Department of Physics, Washington University, St. Louis, MO. 18 Department of Physics and Astronomy, DePauw University, Greencastle, IN. 7 Argonne National Laboratory, Argonne, IL. 19 Department of Physics and Astronomy, Iowa State University, Ames, IA. 8 Department of Physics and Astronomy, University of California, Los 20 Department of Physical and Life Sciences, Galway-Mayo Institute of Angeles, CA. Technology, Dublin Road, Galway, Ireland. 9 School of Physics, University College, Belfield, Dublin, Ireland. 21 NASA Goddard Space Flight Center, Greenbelt, MD. 10 Department of Physics, Purdue University, West Lafayette, IN. 22 Department of Applied Physics and Instrumentation, Cork Institute of 11 Department of Physics, University of Oxford, Oxford, UK. Technology, Bishopstown, Cork, Ireland. 12 Department of Astronomy and Astrophysics, Pennsylvania State Uni- 23 Santa Cruz Institute for Particle Physics and Department of Physics, versity, University Park, PA. University of California, Santa Cruz, CA. 396 VHE OBSERVATIONS OF GRB LOCATIONS 397 this X-ray flare emission has also been predicted (Wang et al. a factor of >100 better than GLAST will achieve (3 photons of 2006). 10 GeV in 104 cm2 collection area). This ignores the large solid- Within the standard fireball shock scenario (Rees & Me´sza´ros angle advantage of a space telescope and the possible steepening 1992; Me´sza´ros&Rees1993;Sarietal.1998),manymodels of the observable spectrum because of the inherent emission mech- have been proposed that predict emission at and above GeVen- anism and the effect of intergalactic absorption by pair produc- ergies during both the prompt and afterglow phases of the GRB. tion. There have been many predictions of high-energy GRB These have been summarized by Zhang & Me´sza´ros (2004 and emission in and above the GeV energy range (Me´sza´ros et al. references therein) and include leptonic models in which gamma 1994; Boettcher & Dermer 1998; Pilla & Loeb 1998; Wang et al. raysareproducedbyelectronselfYinverse Compton emission 2001; Zhang & Me´sza´ros 2001; Guetta & Granot 2003b; Dermer from the internal shocks or from the external forward or reverse & Atoyan 2004; Fragile et al. 2004; see also Zhang & Me´sza´ros shocks. Other models predict gamma rays from proton synchro- 2004 and references therein). tron emission or photomeson cascade emission in the external Until AGILE and GLAST are launched, the GRB observa- shock or from a combination of proton synchrotron emission and tions that were made by the Energetic Gamma-Ray Experiment photomeson cascade emission from internal shocks. Telescope (EGRET) on the Compton Gamma-Ray Observatory Although GRB observations are an important component of (CGRO) will remain the most constraining in the energy range the program at many VHE observatories, correlated observations from30MeVto30GeV.AlthoughEGRETwaslimitedbya at these short wavelengths remain sparse, even though tantaliz- small collection area and large dead time for GRB detection, it ing and inherently very important. The sparsity of observations made sufficient detections to indicate that there is a prompt of GRBs at energies above 10 MeV is dictated not by lack of component with a hard spectrum that extends at least to 100 MeV interest in such phenomena or the absence of theoretical pre- energies. The average spectrum of four bursts detected by EGRET dictions that the emission should occur, but by experimental (GRBs 910503, 930131, 940217, and 940301) did not show any difficulties. evidence for a cutoff up to 10 GeV (Dingus 2001). The relative For the observation of photons of energies above 100 GeV,only insensitivity of EGRETwas such that it was not possible to elim- ground-based telescopes are available at present.
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